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The Galactic O-Star Spectroscopic Survey (GOSSS). III. 142 Additional

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The Galactic O-Star Spectroscopic Survey (GOSSS). III. 142 additional O-type systems1 J. Ma´ızApell´aniz2,3,4,5 Centro de Astrobiolog´ıa, CSIC-INTA, campus ESAC, camino bajo del castillo s/n, E-28 692 Madrid, Spain A. Sota2,3,4 Instituto de Astrof´ısica de Andaluc´ıa-CSIC, Glorieta de la Astronom´ıa s/n, E-18 008 Granada, Spain J. I. Arias, R. H. Barb´a2 Departamento de F´ısica, Universidad de La Serena, Av. Cisternas 1200 Norte, La Serena, Chile N. R. Walborn Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21 218, USA S. Sim´on-D´ıaz Instituto de Astrof´ısica de Canarias, E-38 200 La Laguna, Tenerife, Spain Departamento de Astrof´ısica, Universidad de La Laguna, E-38 205 La Laguna, Tenerife, Spain I. Negueruela DFISTS, EPS, Universidad de Alicante, carretera San Vicente del Raspeig s/n, E-03 690 Alicante, Spain A. Marco DFISTS, EPS, Universidad de Alicante, carretera San Vicente del Raspeig s/n, E-03 690 Alicante, Spain Dept. of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32 611, USA J. R. S. Le˜ao Univ. Federal do Rio Grande do Norte - UFRN, Caixa Postal 1524, CEP 59 078-970, Natal - RN, Brazil A. Herrero Instituto de Astrof´ısica de Canarias, E-38 200 La Laguna, Tenerife, Spain Departamento de Astrof´ısica, Universidad de La Laguna, E-38 205 La Laguna, Tenerife, Spain R. C. Gamen Instituto de Astrof´ısica de La Plata (CONICET, UNLP), Paseo del Bosque s/n, 1900 La Plata, Argentina E. J. Alfaro Instituto de Astrof´ısica de Andaluc´ıa-CSIC, Glorieta de la Astronom´ıa s/n, E-18 008 Granada, Spain ABSTRACT This is the third installment of GOSSS, a massive spectroscopic survey of Galactic O stars, based on new homogeneous, high signal-to-noise ratio, R ∼ 2500 digital observations selected from the Galactic O-Star Catalog (GOSC). In this paper we present 142 additional stellar systems with O stars from both hemispheres, bringing the total of O-type systems published within the project to 590. Among the new objects there are 20 new O stars. We also identify 11 new double-lined arXiv:1602.01336v2 [astro-ph.SR] 8 Feb 2016 spectroscopic binaries (SB2s), of which 6 are of O+O type and 5 of O+B type, and an additional new tripled-lined spectroscopic binary (SB3) of O+O+B type. We also revise some of the previous GOSSS classifications, present some egregious examples of stars erroneously classified as O-type in the past, introduce the use of luminosity class IV at spectral types O4-O5.5, and adapt the classification scheme to the work of Arias et al. (2016). Subject headings: binaries:spectroscopic — binaries:visual — stars:early type — stars:emission line,Be — surveys 1The GOSSS spectroscopic data in this article were William Herschel Telescope (WHT) and 10.4 m Gran Tele- gathered with five facilities: the 1.5 m Telescope at the Ob- scopio Canarias (GTC) at Observatorio del Roque de los servatorio de Sierra Nevada (OSN), the 2.5 m du Pont Tele- Muchachos (ORM). scope at Las Campanas Observatory (LCO), the 3.5 m Tele- 2Visiting Astronomer, LCO, Chile. scope at Calar Alto Observatory (CAHA), and the 4.2 m 3Visiting Astronomer, CAHA, Spain. 1 1. Introduction graph at the Las Campanas (LCO) 2.5 m du Pont telescope). Starting with paper II, some spec- The Galactic O-Star Spectroscopic Survey tra were also obtained with the ISIS spectrograph (GOSSS) is a long-term project that is obtain- at the 4.2 m William Herschel Telescope (WHT) ing homogeneous, high SNR, R ∼ 2500, blue- at the Observatorio del Roque de los Muchachos violet spectra of a large number (1000+) of (ORM) in La Palma, Spain. In this paper we use O stars in the Milky Way and deriving accu- data from all of the above instruments and we also rate and self-consistent spectral types for all of add a new one, OSIRIS, at the 10.4 m Gran Tele- them (Ma´ızApell´aniz et al. 2011). In Sota et al. scopio Canarias (GTC) at the ORM (Table 1). (2011), from now on paper I, we presented the Only a few GTC spectra are used here but the first installment of the survey, which was com- ◦ number will increase in future GOSSS papers, as prised of the results for 178 northern (δ > −20 ) we have already acquired data for over 200 stars, O stars. In Sota et al. (2014), from now on paper most of them too dim to be accessible with the II, we extended the sample to the southern hemi- other telescopes mentioned above. One difference sphere for a total of 448 O stars. Papers I and between the GTC setup and the rest is that we use II concentrated on the brightest O stars with the two volume-phased holographic gratings, R2500U aim of achieving completeness down to B = 8 but and R2500V, allowing us to cover a larger wave- they also included many dimmer stars. This third length range than with the other instruments. The paper continues the previous work by adding 142 exposures for the two gratings are taken consecu- new stars and raising the sample size to 590. Most tively, with the time difference between the first of the new stars are of luminosity class V, which one and the last one being always less than one are relevant to the OVz phenomenon (Arias et al. hour in order to avoid changes in the phase of 2016), but objects of other luminosity classes are rapidly moving spectroscopic binaries. As we do also included. with the rest of the spectrographs, we use checks This paper is organized as follows. We first to compare that the quality of the data from all present the changes in the observational setup and the spectrographs is uniform and, in those cases the classification scheme in section 2. Then, the where the spectral resolution is higher than 2500, spectral classifications are shown in section 3, di- we degrade it to that value. vided in updates to O stars present in papers I We have also started taking GOSSS data with and II, new O stars, and late-type stars previously [a] the GMOS spectrograph at the 8.1 m Gemini misclassified as of O type. Finally, in section 4 we South telescope, [b] the Goodman High Through- analyze the status of the project based on the new put Spectrograph at the 4.1 m SOAR Telescope spectral classifications. (both at Cerro Pach´on, Chile), and [c] FRO- DOspec at the 2.0 m Liverpool Telescope (at the 2. Data and methods ORM) but we do not use them in this paper; their first GOSSS spectra will likely appear in a future 2.1. Blue-violet spectroscopy with R ∼ 2500 paper IV. The GOSSS data were described in papers I and The GOSSS data in this paper were obtained II and the reader is referred there for further in- between 2007 and 2015. The OSN and LCO ob- formation. Here we detail the changes from those servations were obtained in visitor mode, the GTC previous works. observations in service mode, and the CAHA ob- Most of the spectra presented in paper I were servations in a combination of both. For some SB2 obtained with the Albireo (Observatorio de Sierra and SB3 spectroscopic binaries, multiple epochs Nevada - OSN - 1.5 m telescope) and TWIN (Calar were obtained to observe the different orbit phases. Alto - CAHA - 3.5 m telescope) spectrographs. On In cases with known orbits, observations near the other hand, most of the spectra in paper II quadrature were attempted. were obtained with the Boller & Chivens spectro- The spectral classifications which are the main content of this paper are presented in Ta- 4 Visiting Astronomer, WHT, Spain. bles 4, 5, and 6 and they were obtained with MGB 5 e-mail contact: [email protected]. Ma´ızApell´aniz et al. (2012, 2015c). 2 Table 1: Telescopes, instruments, and settings used in this paper. Telescope Spectrograph Grating Spectral scale Spatial scale Wav. range (A/px)˚ (′′/px) (A)˚ LCO 2.5 m (du Pont) Boller & Chivens 1200 0.80 0.71 3900−5500 OSN 1.5 m Albireo 1800 0.62 0.83 3750−5070 CAHA 3.5 m TWIN (blue arm) 1200 0.55 0.58 3930−5020 ORM 4.2 m (WHT) ISIS (blue arm) 600 0.44 0.20 3900−5600 ORM10.4m(GTC) OSIRIS 2500U 0.62 0.25 3440−4610 2500V 0.80 0.25 4500−6000 2.2. Cataloguing 2.3. Spectral classification methodology and the new standard grid The spectral types are available through the lat- est version (currently v3.2) of the Galactic O-Star The spectral classification methodology was Catalog (GOSC, Ma´ızApell´aniz et al. 2004), ac- laid out in paper I and some changes were pre- cessible at http://gosc.iaa.es. Starting in ver- sented in paper II. Here we introduce two addi- sion 3, the GOSSS spectral types are the default tional changes. ones and the basis for the catalog selection, though The first one concerns the OVz phenomenon, older classifications and those obtained with high- described in detail in Sab´ın-Sanjuli´an et al. (2014) resolution spectra are also kept as possible addi- and Arias et al. (2016). OVz stars have deep tional columns. B- and J-band photometry are He ii λ4686 absorption lines, likely caused primar- 1 also provided in GOSC for all stars . The rec- ily by their extreme youth, though additional fac- tified GOSSS spectra can also be obtained from tors may also play a role.
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  • Time, Spatial, and Spectral Resolution of the Halpha Line-Formation Region of Deneb and Rigel with the VEGA/CHARA Interferometer

    Time, Spatial, and Spectral Resolution of the Halpha Line-Formation Region of Deneb and Rigel with the VEGA/CHARA Interferometer

    Astronomy & Astrophysics manuscript no. AB˙Supergiants˙vResubmission˙vEnglishCorr˙Printer c ESO 2018 October 11, 2018 Time, spatial, and spectral resolution of the Hα line-formation region of Deneb and Rigel with the VEGA/CHARA interferometer ⋆ O. Chesneau1, L. Dessart2 D. Mourard1, Ph. B´erio1, Ch. Buil3, D. Bonneau1, M. Borges Fernandes1,9, J.M. Clausse1, O. Delaa1, A. Marcotto1, A. Meilland4, F. Millour4, N. Nardetto1, K. Perraut5, A. Roussel1, A. Spang1, P. Stee1, I. Tallon-Bosc6, H. McAlister7,8, T. ten Brummelaar8, J. Sturmann8, L. Sturmann8, N. Turner8, C. Farrington8 and P.J. Goldfinger8 1 UMR 6525 H. Fizeau, Univ. Nice Sophia Antipolis, CNRS, Observatoire de la Cˆote d’Azur, Av. Copernic, F-06130 Grasse, France 2 Laboratoire d’Astrophysique de Marseille, Universit´ede Provence, CNRS, 38 rue Fr´ed´eric Joliot-Curie, F-13388 Marseille Cedex 13, France 3 Castanet Tolosan Observatory, 6 place Clemence Isaure, 31320 Castanet Tolosan, France 4 Max-Planck Institut f¨ur Radioastronomie, Auf dem Hugel 69, 53121, Bonn, Germany 5 Laboratoire d’Astrophysique de Grenoble (LAOG), Universit´eJoseph-Fourier, UMR 5571 CNRS, BP 53, 38041 Grenoble Cedex 09, France 6 Univ. Lyon 1, Observatoire de Lyon, 9 avenue Charles Andr´e, Saint-Genis Laval, F-69230, France 7 Georgia State University, P.O. Box 3969, Atlanta GA 30302-3969, USA 8 CHARA Array, Mount Wilson Observatory, 91023 Mount Wilson CA, USA 9 Observat´orio Nacional, Rua General Jos´eCristino, 77, 20921-400, S˜ao Cristov˜ao, Rio de Janeiro, Brazil Received, accepted. ABSTRACT Context. BA-type supergiants are amongst the most optically-bright stars.